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We investigate the molecular environment of the Galactic supernova remnant(SNR) Kesteven 78 and perform an XMM-Newton X-ray spectroscopic study for thenortheastern edge of the remnant. SNR Kes78 is found to interact with themolecular clouds (MCs) at a systemic local standard of rest velocity of 81km/s.At around this velocity, the SNR appears to contact a long molecular strip inthe northeast and a large cloud in the east as revealed in the 13CO line, whichmay be responsible for the radio brightness peak and the OH maser,respectively. The 12CO-line bright region morphologically matches the easternbright radio shell in general, and the SNR is consistent in extent with a COcavity. Broadened 12CO line profiles discerned in the eastern maser region andthe western clumpy molecular arc and the elevated 12CO J=2-1/J=1-0 ratios alongthe SNR boundary may be signatures of shock perturbation in the molecular gas.The SNR-MC association places the SNR at a kinematic distance of 4.8 kpc. TheX-rays arising from the northeastern radio shell are emitted by underionizedhot (~1.5 keV), low-density (~0.1 cm^{-3}) plasma with solar abundance, and theplasma may be of intercloud origin. The age of the remnant is inferred to beabout 6 kyr. The size of the molecular cavity in Kes78 implies an initial massaround 22Msun for the progenitor.

Molecular Environment and an X-ray Spectroscopy of Supernova Remnant Kesteven 78